New distances to RAVE stars

ArXiv (2013)

J Binney, B Burnett, G Kordopatis, PJ McMillan, S Sharma, T Zwitter, O Bienayme, J Bland-Hawthorn, M Steinmetz, G Gilmore, MEK Williams, J Navarro, EK Grebel, A Helmi, Q Parker, WA Reid, G Seabroke, F Watson, RFG Wyse

Probability density functions are determined from new stellar parameters for the distance moduli of stars for which the RAdial Velocity Experiment (RAVE) has obtained spectra with S/N>=10. Single-Gaussian fits to the pdf in distance modulus suffice for roughly half the stars, with most of the other half having satisfactory two-Gaussian representations. As expected, early-type stars rarely require more than one Gaussian. The expectation value of distance is larger than the distance implied by the expectation of distance modulus; the latter is itself larger than the distance implied by the expectation value of the parallax. Our parallaxes of Hipparcos stars agree well with the values measured by Hipparcos, so the expectation of parallax is the most reliable distance indicator. The latter are improved by taking extinction into account. The effective temperature absolute-magnitude diagram of our stars is significantly improved when these pdfs are used to make the diagram. We use the method of kinematic corrections devised by Schoenrich, Binney & Asplund to check for systematic errors for general stars and confirm that the most reliable distance indicator is the expectation of parallax. For cool dwarfs and low-gravity giants <pi> tends to be larger than the true distance by up to 30 percent. The most satisfactory distances are for dwarfs hotter than 5500 K. We compare our distances to stars in 13 open clusters with cluster distances from the literature and find excellent agreement for the dwarfs and indications that we are over-estimating distances to giants, especially in young clusters.

Particle Acceleration by Shocks in Supernova Remnants


AR Bell

Erratum: IceCube sensitivity for low-energy neutrinos from nearby supernovae(Astronomy and Astrophysics (2011) 535 : A109 (DOI: 10.1051/0004-6361/201117810))

Astronomy and Astrophysics 563 (2014)

R Abbasi, Y Abdou, T Abu-Zayyad, M Ackermann, J Adams, JA Aguilar, M Ahlers, MM Allen, D Altmann, K Andeen, K Andeen, J Auffenberg, X Bai, X Bai, M Baker, SW Barwick, V Baum, R Bay, JL Bazo Alba, K Beattie, JJ Beatty, JJ Beatty, S Bechet, JK Becker, KH Becker, ML Benabderrahmane, S BenZvi, J Berdermann, P Berghaus, D Berley, E Bernardini, D Bertrand, DZ Besson, D Bindig, M Bissok, E Blaufuss, J Blumenthal, DJ Boersma, C Bohm, D Bose, S Böser, O Botner, AM Brown, S Buitink, KS Caballero-Mora, M Carson, D Chirkin, B Christy, F Clevermann, S Cohen, C Colnard, DF Cowen, DF Cowen, AH Cruz Silva, MV D'Agostino, M Danninger, J Daughhetee, JC Davis, C De Clercq, T Degner, L Demirörs, F Descamps, P Desiati, G De Vries-Uiterweerd, T Deyoung, JC Díaz-Vélez, M Dierckxsens, J Dreyer, JP Dumm, M Dunkman, J Eisch, RW Ellsworth, O Engdegård, S Euler, PA Evenson, O Fadiran, AR Fazely, A Fedynitch, J Feintzeig, T Feusels, K Filimonov, C Finley, T Fischer-Wasels, BD Fox, A Franckowiak, R Franke, TK Gaisser, J Gallagher, L Gerhardt, L Gerhardt, L Gladstone, T Glüsenkamp, A Goldschmidt, JA Goodman, D Góra, D Grant, T Griesel, A Groß, A Groß, S Grullon, M Gurtner, C Ha, A Hajismail, A Hallgren, F Halzen, K Han, K Hanson, K Hanson, D Heinen, K Helbing, R Hellauer, S Hickford, GC Hill, KD Hoffman, B Hoffmann, A Homeier, K Hoshina, W Huelsnitz, W Huelsnitz, JP Hülß, PO Hulth, K Hultqvist, S Hussain, A Ishihara, E Jakobi, J Jacobsen, GS Japaridze, H Johansson, KH Kampert, A Kappes, T Karg, A Karle, P Kenny, J Kiryluk, J Kiryluk, F Kislat, SR Klein, SR Klein, H Köhne, G Kohnen, H Kolanoski, L Köpke, S Kopper, DJ Koskinen, M Kowalski, T Kowarik, M Krasberg, G Kroll, N Kurahashi, T Kuwabara, M Labare, K Laihem, H Landsman, MJ Larson, R Lauer, J Lünemann, J Madsen, A Marotta, R Maruyama, K Mase, HS Matis, K Meagher, M Merck, P Mészáros, P Mészáros, T Meures, S Miarecki, S Miarecki, E Middell, N Milke, J Miller, T Montaruli, T Montaruli, R Morse, SM Movit, R Nahnhauer, JW Nam, U Naumann, DR Nygren, S Odrowski, A Olivas, M Olivo, M Olivo, A O'murchadha, S Panknin, L Paul, CP De Los Heros, J Petrovic, A Piegsa, D Pieloth, R Porrata, J Posselt, PB Price, GT Przybylski, K Rawlins, P Redl, E Resconi, E Resconi, E Resconi, W Rhode, M Ribordy, AS Richard, M Richman, JP Rodrigues, F Rothmaier, C Rott, T Ruhe, D Rutledge, B Ruzybayev, D Ryckbosch, HG Sander, M Santander, S Sarkar, K Schatto, T Schmidt, A Schönwald, A Schukraft, L Schulte, A Schultes, O Schulz, O Schulz, M Schunck, D Seckel, B Semburg, SH Seo, Y Sestayo, S Seunarine, A Silvestri, K Singh, A Slipak, GM Spiczak, C Spiering, M Stamatikos, M Stamatikos, T Stanev, T Stezelberger, RG Stokstad, A Stößl, EA Strahler, R Ström, M Stüer, GW Sullivan, Q Swillens, H Taavola, I Taboada, A Tamburro, A Tepe, S Ter-Antonyan, S Tilav, PA Toale, S Toscano, D Tosi, N Van Eijndhoven, J Vandenbroucke, A Van Overloop, J Van Santen, M Vehring, M Voge, C Walck, T Waldenmaier, M Wallraff, M Walter, C Weaver, C Wendt, S Westerhoff, N Whitehorn, K Wiebe, CH Wiebusch, DR Williams, R Wischnewski, H Wissing, M Wolf, TR Wood, K Woschnagg, C Xu, DL Xu, XW Xu, JP Yanez, G Yodh, S Yoshida, P Zarzhitsky, M Zoll

How the cosmic web induces intrinsic alignments of galaxies

ArXiv (2014)

S Codis, Y Dubois, C Pichon, J Devriendt, A Slyz

Intrinsic alignments are believed to be a major source of systematics for future generation of weak gravitational lensing surveys like Euclid or LSST. Direct measurements of the alignment of the projected light distribution of galaxies in wide field imaging data seem to agree on a contamination at a level of a few per cent of the shear correlation functions, although the amplitude of the effect depends on the population of galaxies considered. Given this dependency, it is difficult to use dark matter-only simulations as the sole resource to predict and control intrinsic alignments. We report here estimates on the level of intrinsic alignment in the cosmological hydrodynamical simulation Horizon-AGN that could be a major source of systematic errors in weak gravitational lensing measurements. In particular, assuming that the spin of galaxies is a good proxy for their ellipticity, we show how those spins are spatially correlated and how they couple to the tidal field in which they are embedded. We also present theoretical calculations that illustrate and qualitatively explain the observed signals.

A current driven electromagnetic mode in sheared and toroidal configurations

ArXiv (2013)

I Pusztai, PJ Catto, FI Parra, M Barnes

The induced electric field in a tokamak drives a parallel electron current flow. In an inhomogeneous, finite beta plasma, when this electron flow is comparable to the ion thermal speed, the Alfven mode wave solutions of the electromagnetic gyrokinetic equation can become nearly purely growing kink modes. Using the new "low-flow" version of the gyrokinetic code GS2 developed for momentum transport studies [Barnes et al 2013 Phys. Rev. Lett. 111, 055005], we are able to model the effect of the induced parallel electric field on the electron distribution to study the destabilizing influence of current on stability. We identify high mode number kink modes in GS2 simulations and make comparisons to analytical theory in sheared magnetic geometry. We demonstrate reassuring agreement with analytical results both in terms of parametric dependences of mode frequencies and growth rates, and regarding the radial mode structure.

Letter of Intent: The Precision IceCube Next Generation Upgrade (PINGU)

ArXiv (2014)

TI-P Collaboration

The Precision IceCube Next Generation Upgrade (PINGU) is a proposed low-energy in-fill extension to the IceCube Observatory. With detection technology modeled closely on the successful IceCube example, PINGU will feature the world's largest effective volume for neutrinos at an energy threshold of a few GeV, enabling it to reach its chief goal of determining the neutrino mass hierarchy (NMH) quickly and at modest cost. PINGU will be able to distinguish between the normal and inverted NMH at $3\sigma$ significance with an estimated 3.5 years of data. With its unprecedented statistical sample of low energy atmospheric neutrinos, PINGU will also have highly competitive sensitivity to $\nu_\mu$ disappearance, $\theta_{23}$ octant and maximal mixing, and $\nu_\tau$ appearance. PINGU can also extend the search for solar WIMP dark matter into the region currently favored by some direct dark matter experiments. At the lower end of the energy range, PINGU can use neutrino tomography to perform the first-ever direct measurement of the composition of the Earth's core. With its increased module density, PINGU will improve IceCube's sensitivity to galactic supernova neutrino bursts and enable it to extract the neutrino energy spectral shape.

The Gaia-ESO Survey: The analysis of high-resolution UVES spectra of FGK-type stars


R Smiljanic, AJ Korn, M Bergemann, A Frasca, L Magrini, T Masseron, E Pancino, G Ruchti, I San Roman, L Sbordone, SG Sousa, H Tabernero, G Tautvaisiene, M Valentini, M Weber, CC Worley, VZ Adibekyan, C Allende Prieto, G Barisevicius, K Biazzo, S Blanco-Cuaresma, P Bonifacio, A Bragaglia, E Caffau, T Cantat-Gaudin, Y Chorniy, P de Laverny, E Delgado-Mena, P Donati, S Duffau, E Franciosini, E Friel, D Geisler, JI Gonzalez Hernandez, P Gruyters, G Guiglion, CJ Hansen, U Heiter, V Hill, HR Jacobson, P Jofre, H Jonsson, AC Lanzafame, C Lardo, H-G Ludwig, E Maiorca, S Mikolaitis, D Montes, T Morel, A Mucciarelli, C Munoz, T Nordlander, L Pasquini, E Puzeras, A Recio-Blanco, N Ryde, G Sacco, NC Santos, AM Serenelli, R Sordo, C Soubiran, L Spina, M Steffen, A Vallenari, S Van Eck, S Villanova, G Gilmore, S Randich, M Asplund, J Binney, J Drew, S Feltzing, A Ferguson, R Jeffries, G Micela, I Negueruela, T Prusti, H-W Rix, E Alfaro, C Babusiaux, T Bensby, R Blomme, E Flaccomio, P Francois, M Irwin, S Koposov, N Walton, A Bayo, G Carraro, MT Costado, F Damiani, B Edvardsson, A Hourihane, R Jackson, J Lewis, K Lind, G Marconi, C Martayan, L Monaco, L Morbidelli, L Prisinzano, S Zaggia

Why do galactic spins flip in the cosmic web? A Theory of Tidal Torques near saddles

ArXiv (2014)

C Pichon, S Codis, D Pogosyan, Y Dubois, V Desjacques, J Devriendt

Filaments of the cosmic web drive spin acquisition of disc galaxies. The point process of filament-type saddle represent best this environment and can be used to revisit the Tidal Torque Theory in the context of an anisotropic peak (saddle) background split. The constrained misalignment between the tidal tensor and the Hessian of the density field generated in the vicinity of filament saddle points simply explains the corresponding transverse and longitudinal point-reflection symmetric geometry of spin distribution. It predicts in particular an azimuthal orientation of the spins of more massive galaxies and spin alignment with the filament for less massive galaxies. Its scale dependence also allows us to relate the transition mass corresponding to the alignment of dark matter halos spin relative to the direction of their neighboring filament to this geometry, and to predict accordingly it s scaling with the mass of non linearity, as was measured in simulations.

Models of magnetic field evolution and effective viscosity in weakly collisional extragalactic plasmas


F Mogavero, AA Schekochihin

Modelling gamma-ray photon emission and pair production in high-intensity laser-matter interactions

Journal of Computational Physics 260 (2014) 273-285

CP Ridgers, CP Ridgers, CP Ridgers, JG Kirk, R Duclous, TG Blackburn, CS Brady, K Bennett, TD Arber, AR Bell, AR Bell

In high-intensity (>1021 Wcm -2) laser-matter interactions gamma-ray photon emission by the electrons can strongly affect the electron's dynamics and copious numbers of electron-positron pairs can be produced by the emitted photons. We show how these processes can be included in simulations by coupling a Monte Carlo algorithm describing the emission to a particle-in-cell code. The Monte Carlo algorithm includes quantum corrections to the photon emission, which we show must be included if the pair production rate is to be correctly determined. The accuracy, convergence and energy conservation properties of the Monte Carlo algorithm are analysed in simple test problems. © 2013 Elsevier Inc.

High energy conversion efficiency in laser-proton acceleration by controlling laser-energy deposition onto thin foil targets

Applied Physics Letters 104 (2014)

CM Brenner, CM Brenner, APL Robinson, K Markey, RHH Scott, RJ Gray, M Rosinski, O Deppert, J Badziak, D Batani, JR Davies, SM Hassan, KL Lancaster, K Li, IO Musgrave, PA Norreys, PA Norreys, J Pasley, J Pasley, M Roth, HP Schlenvoigt, C Spindloe, M Tatarakis, T Winstone, J Wolowski, D Wyatt, P McKenna, D Neely

An all-optical approach to laser-proton acceleration enhancement is investigated using the simplest of target designs to demonstrate application-relevant levels of energy conversion efficiency between laser and protons. Controlled deposition of laser energy, in the form of a double-pulse temporal envelope, is investigated in combination with thin foil targets in which recirculation of laser-accelerated electrons can lead to optimal conditions for coupling laser drive energy into the proton beam. This approach is shown to deliver a substantial enhancement in the coupling of laser energy to 5-30 MeV protons, compared to single pulse irradiation, reaching a record high 15% conversion efficiency with a temporal separation of 1 ps between the two pulses and a 5 μm-thick Au foil. A 1D simulation code is used to support and explain the origin of the observation of an optimum pulse separation of ∼1 ps. © 2014 Author(s).

A current driven electromagnetic mode in sheared and toroidal configurations (vol 56, 035011, 2014)


I Pusztai, PJ Catto, FI Parra, M Barnes

Comparison of BES measurements of ion-scale turbulence with direct gyro-kinetic simulations of MAST L-mode plasmas

Plasma Physics and Controlled Fusion 56 (2014)

AR Field, D Dunai, YC Ghim, YC Ghim, P Hill, B McMillan, CM Roach, S Saarelma, AA Schekochihin, S Zoletnik

Observations of ion-scale (kyρi 1) density turbulence of relative amplitude 0.2% are available on the Mega Amp Spherical Tokamak (MAST) using a 2D (8 radial × 4 poloidal channel) imaging beam emission spectroscopy diagnostic. Spatial and temporal characteristics of this turbulence, i.e., amplitudes, correlation times, radial and perpendicular correlation lengths and apparent phase velocities of the density contours, are determined by means of correlation analysis. For a low-density, L-mode discharge with strong equilibrium flow shear exhibiting an internal transport barrier in the ion channel, the observed turbulence characteristics are compared with synthetic density turbulence data generated from global, non-linear, gyro-kinetic simulations using the particle-in-cell code NEMORB. This validation exercise highlights the need to include increasingly sophisticated physics, e.g., kinetic treatment of trapped electrons, equilibrium flow shear and collisions, to reproduce most of the characteristics of the observed turbulence. Even so, significant discrepancies remain: an underprediction by the simulations of the turbulence amplitude and heat flux at plasma periphery and the finding that the correlation times of the numerically simulated turbulence are typically two orders of magnitude longer than those measured in MAST. Comparison of these correlation times with various linear timescales suggests that, while the measured turbulence is strong and may be 'critically balanced', the simulated turbulence is weak. © 2014 IOP Publishing Ltd.

Firehose and Mirror Instabilities in a Collisionless Shearing Plasma


MW Kunz, AA Schekochihin, JM Stone

Effect on plasma rotation of lower hybrid (LH) waves in Alcator C-Mod

AIP Conference Proceedings 1580 (2014) 398-401

JP Lee, M Barnes, RR Parker, JE Rice, FI Parra, PT Bonoli, ML Reinke

The injection of LH waves for current drive into a tokamak changes the ion toroidal rotation. In Alcator C-Mod, the direction of the steady state rotation change due to LH waves depends on the plasma current and the density. The change in rotation can be estimated by balancing the external torque of lower hybrid waves with the turbulent radial transport of the momentum. For high plasma current, the turbulent pinch and diffusion of the injected counter-current momentum are sufficient to explain the rotation change. However, for low plasma current, the change in the the intrinsic momentum transport (residual stress) for a non-rotating state is required to explain the co-current rotation change. Accordingly, we investigate the intrinsic momentum transport for the non-rotating state when diamagnetic flow and ExB flow cancel each other. The change in the intrinsic momentum transport due to lower hybrid waves is significant when the plasma current is low, which may explain the rotation reversal for low plasma current. The effect of changed q (safety factor) profile by lower hybrid on the intrinsic momentum transport is estimated by gyrokinetics. © 2014 AIP Publishing LLC.

Long-wavelength limit of gyrokinetics in a turbulent tokamak and its intrinsic ambipolarity

ArXiv (2012)

I Calvo, FI Parra

Recently, the electrostatic gyrokinetic Hamiltonian and change of coordinates have been computed to order $\epsilon^2$ in general magnetic geometry. Here $\epsilon$ is the gyrokinetic expansion parameter, the gyroradius over the macroscopic scale length. Starting from these results, the long-wavelength limit of the gyrokinetic Fokker-Planck and quasineutrality equations is taken for tokamak geometry. Employing the set of equations derived in the present article, it is possible to calculate the long-wavelength components of the distribution functions and of the poloidal electric field to order $\epsilon^2$. These higher-order pieces contain both neoclassical and turbulent contributions, and constitute one of the necessary ingredients (the other is given by the short-wavelength components up to second order) that will eventually enter a complete model for the radial transport of toroidal angular momentum in a tokamak in the low flow ordering. Finally, we provide an explicit and detailed proof that the system consisting of second-order gyrokinetic Fokker-Planck and quasineutrality equations leaves the long-wavelength radial electric field undetermined; that is, the turbulent tokamak is intrinsically ambipolar.

When omnigeneity fails

ArXiv (2014)

FI Parra, I Calvo, JL Velasco, JA Alonso

A generic non-symmetric magnetic field does not confine magnetized charged particles for long times due to secular magnetic drifts. Stellarator magnetic fields should be omnigeneous (that is, designed such that the secular drifts vanish), but perfect omnigeneity is technically impossible. There always are small deviations from omnigeneity that necessarily have large gradients. The amplification of the energy flux caused by a deviation of size $\epsilon$ is calculated and it is shown that the scaling with $\epsilon$ of the amplification factor can be as large as linear. In opposition to common wisdom, most of the transport is not due to particles trapped in ripple wells, but to the perturbed motion of particles trapped in the omnigeneous magnetic wells around their bounce points.

Quantum theory of Thomson scattering


BJB Crowley, G Gregori

AMS-02 data confronts acceleration of cosmic ray secondaries in nearby sources

ArXiv (2014)

P Mertsch, S Sarkar

We revisit the model proposed earlier to account for the observed increase in the positron fraction in cosmic rays with increasing energy, in the light of new data from the Alpha Magnetic Spectrometer (AMS-02) experiment. The model accounts for the production and acceleration of secondary electrons and positrons in nearby supernova remnants which results in an additional, harder component that becomes dominant at high energies. By fitting this to AMS-02 data we can calculate the expected concomitant rise of the boron-to-carbon ratio, as well as of the fraction of antiprotons. If these predictions are confirmed by the forthcoming AMS-02 data it would conclusively rule out all other proposed explanations, in particular dark matter annihilations or decays.



H Liu, P Mertsch, S Sarkar